Sunspot
View article: Solar Cycle Variation of Sustained Gamma Ray Emission from the Sun
Solar Cycle Variation of Sustained Gamma Ray Emission from the Sun Open
We investigated the occurrence rate of the sustained gamma ray emission (SGRE) events from the Sun using data obtained by the Large Area Telescope (LAT) on board the Fermi satellite since its launch in 2008. The data cover the whole of sol…
View article: Sympathetic Eruption of Two Filaments and Associated Solar Coronal Jet
Sympathetic Eruption of Two Filaments and Associated Solar Coronal Jet Open
Combining the high-quality observations from the Solar Dynamics Observatory, the Global Oscillation Network Group, and the Chinese H α Solar Explorer, we report a solar coronal jet triggered by the sympathetic eruption of two filaments on …
View article: The calm before the storm: High spatial resolution mosaic of active region NOAA 14274 at the onset of an X1.2 flare
The calm before the storm: High spatial resolution mosaic of active region NOAA 14274 at the onset of an X1.2 flare Open
Active region NOAA 14274 produced some of the strongest flares of Solar Cycle 25, including the X1.2 and X5.1 flares on 10 and 11 November 2025, respectively. We present the first large mosaic of speckle-restored images obtained with the i…
View article: Fractal-Unified Field Theory Characterization of NOAA Active Region 4274: A 5D Fractal Aether Analysis of the Most Explosive Sunspot Complex of Solar Cycle 25 (November 2025).
Fractal-Unified Field Theory Characterization of NOAA Active Region 4274: A 5D Fractal Aether Analysis of the Most Explosive Sunspot Complex of Solar Cycle 25 (November 2025). Open
"NOAA Active Region 4274 (November 2025) produced at least five X-class flares within two weeks, including the strongest of the year (X5.1 on Nov 11) and a terminal limb-discharge X4.0 flare on Nov 14. Using the 5D Fractal-Unified Field Th…
View article: Fractal-Unified Field Theory Characterization of NOAA Active Region 4274: A 5D Fractal Aether Analysis of the Most Explosive Sunspot Complex of Solar Cycle 25 (November 2025).
Fractal-Unified Field Theory Characterization of NOAA Active Region 4274: A 5D Fractal Aether Analysis of the Most Explosive Sunspot Complex of Solar Cycle 25 (November 2025). Open
"NOAA Active Region 4274 (November 2025) produced at least five X-class flares within two weeks, including the strongest of the year (X5.1 on Nov 11) and a terminal limb-discharge X4.0 flare on Nov 14. Using the 5D Fractal-Unified Field Th…
View article: Solar STFO v2.1: Tau-Saturated Stellar Dynamics, Hemispheric Asymmetry, and Planetary Honing
Solar STFO v2.1: Tau-Saturated Stellar Dynamics, Hemispheric Asymmetry, and Planetary Honing Open
Solar STFO v2.1 is a refined scalar-temporal-field model of the solar magneticcycle incorporating two new physically essential components: (1) tau-fieldsaturation inside stellar interiors, and (2) a hemispherically asymmetrictau-density pr…
View article: Solar STFO v2.1: Tau-Saturated Stellar Dynamics, Hemispheric Asymmetry, and Planetary Honing
Solar STFO v2.1: Tau-Saturated Stellar Dynamics, Hemispheric Asymmetry, and Planetary Honing Open
Solar STFO v2.1 is a refined scalar-temporal-field model of the solar magneticcycle incorporating two new physically essential components: (1) tau-fieldsaturation inside stellar interiors, and (2) a hemispherically asymmetrictau-density pr…
View article: Statistical Overview of Long-lived Active Regions Observed across Multiple Carrington Rotations
Statistical Overview of Long-lived Active Regions Observed across Multiple Carrington Rotations Open
The study of solar active regions (ARs) is of central importance to a range of fundamental science, as well as the practical applications of space weather. AR emergence and life cycles are two areas of particular interest, yet the lack of …
View article: The Calm before the Storm: High Spatial Resolution Mosaic of Active Region NOAA 14274 at the Onset of an X1.2 Flare
The Calm before the Storm: High Spatial Resolution Mosaic of Active Region NOAA 14274 at the Onset of an X1.2 Flare Open
Active region NOAA 14274 produced some of the strongest flares of Solar Cycle 25, including the X1.2 and X5.1 flares on 2025 November 10 and 11, respectively. We present the first large mosaic of speckle-restored images obtained with the i…
View article: Historical Reconstruction of Solar Surface Magnetism from Cycle 1-24 Using the Synthetic Active Region Generator (SARG) and the Advective Flux Transport (AFT) Model
Historical Reconstruction of Solar Surface Magnetism from Cycle 1-24 Using the Synthetic Active Region Generator (SARG) and the Advective Flux Transport (AFT) Model Open
The historical reconstruction of the Sun's surface magnetic field remains a persistent challenge, limiting our ability to investigate the long-term global properties of the Sun, including the evolution of the large-scale magnetic field, so…
View article: Historical Reconstruction of Solar Surface Magnetism from Cycle 1-24 Using the Synthetic Active Region Generator (SARG) and the Advective Flux Transport (AFT) Model
Historical Reconstruction of Solar Surface Magnetism from Cycle 1-24 Using the Synthetic Active Region Generator (SARG) and the Advective Flux Transport (AFT) Model Open
The historical reconstruction of the Sun's surface magnetic field remains a persistent challenge, limiting our ability to investigate the long-term global properties of the Sun, including the evolution of the large-scale magnetic field, so…
View article: On the planetary forcing of the Solar dynamo: Evidence from a Lagrangian framework
On the planetary forcing of the Solar dynamo: Evidence from a Lagrangian framework Open
Whether planetary motions influence the solar magnetic cycle has remained an open question due to the lack of a rigorous physical mechanism. Here we develop a Lagrangian framework based on the Virial theorem to show that planetary orbital …
View article: Centennial solar EUV irradiance from ionospheric currents: Varying sunspot-EUV irradiance relation and modified spot-facula ratio
Centennial solar EUV irradiance from ionospheric currents: Varying sunspot-EUV irradiance relation and modified spot-facula ratio Open
Sunspots depict large variability during the last 100 years, a period called the Modern Maximum (MM). However, other variables are needed to study the long-term evolution, e.g., of weaker fields and different radiative emissions. Recently,…
View article: On the planetary forcing of the Solar dynamo: Evidence from a Lagrangian framework
On the planetary forcing of the Solar dynamo: Evidence from a Lagrangian framework Open
Whether planetary motions influence the solar magnetic cycle has remained an open question due to the lack of a rigorous physical mechanism. Here we develop a Lagrangian framework based on the Virial theorem to show that planetary orbital …
View article: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations Open
Solar wind backmapping is a critical technique for analyzing the origin of the solar wind and space weather events by correlating in situ measurements with solar remote-sensing observations. This technique typically traces magnetic field l…
View article: Characteristics of Magnetic Field Evolution and Onset Process of Successive X-class Flares in May 2024
Characteristics of Magnetic Field Evolution and Onset Process of Successive X-class Flares in May 2024 Open
In early May 2024, active regions (ARs) 13663 and 13664 appeared on the solar disk and produced 17 X-class flares. The associated coronal mass ejections caused geomagnetic disturbances, named the Gannon Storm, resulting in significant soci…
View article: Coronal Heating Problem from the Generative Kernel: Local Coherence Avalanches in the Solar Atmosphere
Coronal Heating Problem from the Generative Kernel: Local Coherence Avalanches in the Solar Atmosphere Open
The solar corona is millions of degrees hotter than the photosphere — a persistent 70-year astrophysical paradox. Within Relational Field Theory (RFT), the mystery dissolves. The universe is governed by a single bounded coherence scalar R_…
View article: Coronal Heating Problem from the Generative Kernel: Local Coherence Avalanches in the Solar Atmosphere
Coronal Heating Problem from the Generative Kernel: Local Coherence Avalanches in the Solar Atmosphere Open
The solar corona is millions of degrees hotter than the photosphere — a persistent 70-year astrophysical paradox. Within Relational Field Theory (RFT), the mystery dissolves. The universe is governed by a single bounded coherence scalar R_…
View article: Probing Starspot Dynamics on the Active M Dwarf TIC 272272592: A Multiyear TESS Study
Probing Starspot Dynamics on the Active M Dwarf TIC 272272592: A Multiyear TESS Study Open
We present an analysis of temporal starspot evolution and its distribution on an active rapid rotator ( P rot = 1.22 days), TIC 272272592, using high-precision time-series photometry from the Transiting Exoplanet Survey Satellite spanning …
View article: Observed Joy’s Law of Bipolar Magnetic Region Tilts at Emergence Supports the Thin Flux Tube Model
Observed Joy’s Law of Bipolar Magnetic Region Tilts at Emergence Supports the Thin Flux Tube Model Open
Bipolar sunspots, or more generally, bipolar magnetic regions (BMRs), are the dynamic magnetic regions that appear on the solar surface and are central to solar activity. One striking feature of these regions is that they are often tilted …
View article: Solar Wind Dynamic Pressure and Its Correlation with Cosmic Ray Flux Variability at Earth
Solar Wind Dynamic Pressure and Its Correlation with Cosmic Ray Flux Variability at Earth Open
The solar wind dynamic pressure is one of the most fundamental parameters that characterize the energy and momentum flux carried by the solar wind plasma. It directly affects the structure and dynamics of the interplanetary magnetic field …
View article: Solar Filament Physiognomy: Inferring Magnetic Quantities from Imaging Observations
Solar Filament Physiognomy: Inferring Magnetic Quantities from Imaging Observations Open
Magnetic field is the key physical quantity in solar physics as it controls all kinds of solar activity, ranging from nanoflares to big flares and coronal mass ejections (CMEs). However, so far only the magnetic field on the solar surface …
View article: Solar Filament Physiognomy: Inferring Magnetic Quantities from Imaging Observations
Solar Filament Physiognomy: Inferring Magnetic Quantities from Imaging Observations Open
Magnetic field is the key physical quantity in solar physics as it controls all kinds of solar activity, ranging from nanoflares to big flares and coronal mass ejections (CMEs). However, so far only the magnetic field on the solar surface …
View article: Solar Cycle 25 Dynamics from Observational and Statistical Parameters: Characterization of the Maximum Phase and Rotational Behaviour
Solar Cycle 25 Dynamics from Observational and Statistical Parameters: Characterization of the Maximum Phase and Rotational Behaviour Open
We present a comprehensive analysis of Solar Cycle 25 aimed at precisely constraining the interval of its activity maximum using multiple observational parameters: sunspot number (SSN), Wolf number, the 10.7 cm solar radio flux (F10.7), th…
View article: Solar Cycle 25 Dynamics from Observational and Statistical Parameters: Characterization of the Maximum Phase and Rotational Behaviour
Solar Cycle 25 Dynamics from Observational and Statistical Parameters: Characterization of the Maximum Phase and Rotational Behaviour Open
We present a comprehensive analysis of Solar Cycle 25 aimed at precisely constraining the interval of its activity maximum using multiple observational parameters: sunspot number (SSN), Wolf number, the 10.7 cm solar radio flux (F10.7), th…
View article: A Mid-latitude Non-detection of a Magnetic Crochet during the 2025 November 4 X1.8 Solar Flare
A Mid-latitude Non-detection of a Magnetic Crochet during the 2025 November 4 X1.8 Solar Flare Open
I investigated the near-Earth response to the 2025 November 4 X1.8 solar flare (peak 17:34 UT) using seven days of GOES-18 soft X-ray, integral proton, and magnetometer data, together with one-minute scalar geomagnetic measurements from US…
View article: The Formation of Solar Prominences: Plasma Origin and Mechanisms
The Formation of Solar Prominences: Plasma Origin and Mechanisms Open
Solar prominences, or solar filaments, are cool and dense plasma structures in the hot solar corona, whose formation mechanisms have remained a fundamental challenge in solar physics. This review provides a comprehensive overview of the cu…
View article: Vilnius Dallmeyer Photoheliograph Solar Archive (1869–1874): Digital Collection of 283 Surviving Photographs
Vilnius Dallmeyer Photoheliograph Solar Archive (1869–1874): Digital Collection of 283 Surviving Photographs Open
This repository contains the complete set of 283 surviving solar photographs obtained with the Vilnius Dallmeyer photoheliograph, the second photoheliograph in the world and the first constructed by John Henry Dallmeyer, taken between 1869…
View article: The Formation of Solar Prominences: Plasma Origin and Mechanisms
The Formation of Solar Prominences: Plasma Origin and Mechanisms Open
Solar prominences, or solar filaments, are cool and dense plasma structures in the hot solar corona, whose formation mechanisms have remained a fundamental challenge in solar physics. This review provides a comprehensive overview of the cu…
View article: Influence of Magnetic Complexity of Active Regions on Solar Wind Properties during Solar Cycles 23 and 24
Influence of Magnetic Complexity of Active Regions on Solar Wind Properties during Solar Cycles 23 and 24 Open
Linking the properties of solar wind to the activity and characteristics of its source regions can enhance our understanding of its origin and generation mechanisms. Using the Mount Wilson magnetic classification, we categorize all active …